LOGIN TO YOUR ACCOUNT

Username
Password
Remember Me
Or use your Academic/Social account:

CREATE AN ACCOUNT

Or use your Academic/Social account:

Congratulations!

You have just completed your registration at OpenAire.

Before you can login to the site, you will need to activate your account. An e-mail will be sent to you with the proper instructions.

Important!

Please note that this site is currently undergoing Beta testing.
Any new content you create is not guaranteed to be present to the final version of the site upon release.

Thank you for your patience,
OpenAire Dev Team.

Close This Message

CREATE AN ACCOUNT

Name:
Username:
Password:
Verify Password:
E-mail:
Verify E-mail:
*All Fields Are Required.
Please Verify You Are Human:
fbtwitterlinkedinvimeoflicker grey 14rssslideshare1
Hughes, Thomas Marcus
Languages: English
Types: Doctoral thesis
Subjects: QC

Classified by OpenAIRE into

arxiv: Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
The main aims of this thesis are: (a) an investigation into the evolutionary histories of nearby galaxies, via the use of ultraviolet-infrared colour-mass diagrams, to uncover the dominant mechanism driving nearby galaxy evolution; (b) the determination of the impact of feedback from active galactic nuclei on star formation; and (c) a study of chemical evolution of star-forming galaxies in different environments. The analysis confirms recent observations of a population of late-type galaxies with reduced levels of star formation. I demonstrate that feedback from active nuclei is unlikely to be the dominant mechanism quenching star formation and driving the evolution of thee late-type galaxies. In fact, galaxies with quenched star formation are typically gas-deficient cluster galaxies, suggesting that environmental effects are responsible for removing the gas required to fuel star formation. A fraction of quenched late-type galaxies are, however, not gas deficient, and form a more heterogeneous class of objects with more complex evolutionary histories. On the other hand, the chemical evolution of star-forming galaxies, as traced by the stellar mass-metallicity relation, is shown to be invariant with environment, suggesting that internal processes drive chemical evolution. The clear observational evidence presented here indicates that, in the concordance model of galaxy formation and evolution, environmental effects must be taken into account in order to gain a better understanding of galaxy evolution in the local universe.
  • The results below are discovered through our pilot algorithms. Let us know how we are doing!

    • 2 T h e H R S + Sam ple 2 . 1 The Herschel Reference Survey .................................................................. 2.2 Selection c r i t e r i a ............................................................................................ 2.3 Mutliwavelength o b s e rv a tio n s ..................................................................... 2.3.1 Summary of observations.................................................................. 2.4 Derived physical p ro p erties........................................................................... 2.4.1 Stellar m a s s ......................................................................................... 2.4.2 Hi mass and deficien cy...................................................................... 2.4.3 Classification of nuclear a c tiv ity ..................................................... 2.5 C o n c lu s io n s ......................................................................................................
    • 3 U ltra v io let P h o to m e tr y 3.1 In tro d u c tio n ...................................................................................................... 3.2 The Galaxy Evolution E x p lo r e r ................................................................. 3.3 UV observations............................................................................................... 3.4 A perture p h o to m e try ..................................................................................... 3.5 Dust attenuation corrections . ................................................................. 3.6 Star formation rates ..................................................................................... 3.7 C o n c lu s io n s .....................................................................................................
    • 5.1 In tro d u c tio n .........................................................................................................
    • 5.2 The colour-mass d ia g ra m ..................................................................................
    • 5.3 The link between Hi content and c o lo u r......................................................
    • 5.4 Defining the transition r e g i o n .......................................................................
    • 5.5 The properties of transition galax ies............................................................. 5.5.1 Hi-deficient sy ste m s............................................................................... 5.5.2 Hi-normal g a l a x i e s ...............................................................................
    • 5.6 Discussion &; c o n clu sio n s.................................................................................. 5.6.1 The m igration of Hi-deficient g a la x ie s........................................... 5.6.2 The Hi-normal transition g a la x ie s .................................................
    • 6.1 In tro d u c tio n .........................................................................................................
    • 6 . 2 Sample c a v e a t......................................................................................................
    • 6.3 Surface p h o to m e try ............................................................................................
    • 6.4 Ultraviolet-infrared colour p ro file s .................................................................
    • 6.5 Variation in isophotal r a d i i ..............................................................................
    • 6 . 6 C o n c lu sio n s.........................................................................................................
    • 10 D iscu ssio n &: C onclusions 10.1 O verview ............................................................................................................. 1 0 . 2 Key results ...................................................................................................... 10.3 Constraints on galaxy e v o lu tio n .................................................................. 10.3.1 Star formation on the blue cloud .................................................. 10.3.2 Migration from the blue c l o u d ........................................................ 10.3.3 Evolution from the red sequence..................................................... 10.4 Final conclu sio n ................................................................................................ 10.5 Future w o r k ......................................................................................................
    • 4.1 The reddening function f(A) of Lequeux et al. (1979), which is based on the extinction law of W hitford (1958), adopted for the extinction corrections relative to H/?.................................................................................
    • 5.1 The properties of Hi-normal transition and red-sequence galaxies in the HRS+ s a m p le .............................................................................................
    • 7.1 The values assumed for various param eters used in the toy analytic model of AGN feedback ...............................................................................
    • 9.1 Properties of the 23 galaxies with D02-based metallicities 12+ log(0/H ) > 8.9, all of which display nuclear a c t i v i t y ............................................... 167
    • 9.2 The coefficients and xl values given by linear and polynomial leastsquares fits to the total sample in the mass-metallicity p l o t s ............. 168
    • 9.3 The coefficients and x l values given by linear and polynomial leastsquares fits to the observations of galaxies in different environments in the m ass-metallicity plots ............................................................................ 172
    • C .l Measured Ci values and corrected emission line intensities, normalised to the H a i n t e n s i t y ......................................................................................... 254
    • 1 . 1 The morphological classification scheme of galaxies ...............................
    • 1 . 2 The unified model of active galactic n u c l e i ...............................................
    • 1.3 The observed K-band luminosity function of galaxies in the local Universe compared to theoretical predictions, with and w ithout AGN feedback ....................................................................................................................
    • 2 . 1 The sky distribution of the HRS+ galaxies, with a magnified view of the Virgo cluster reg io n ...................................................................................
    • 2.2 A comparison of the morphological type and K band luminosity distributions for the HRS and HRS+ s a m p le s ...............................................
    • 2.3 The completeness of observations of HRS+ galaxies in the FUV, NUV and B b a n d s .......................................................................................................
    • 2.3 The completeness of HRS-t- galaxies imaged in the V band, and with optical spectroscopy and Hi line m easurem ents........................................
    • 2.4 The B PT diagnostic diagram used to classify the spectra of galaxies in this w o rk .............................................................................................................
    • 3.1 A GALEX NUV band image of VCC1043
    • 3.2 A comparison between FUV and NUV magnitudes measured via aperture photometry, for which multiple observations are available . . . .
    • 3.3 A comparison between the FUV and NUV magnitudes measured in this work to measurements made in previous s tu d ie s ..............................
    • 3.4 The completeness of HRS+ galaxies observed in the ultraviolet bands
    • 4.1 The spectroscopic coverage of the late-type galaxies in the H R S+ sample 46
    • 4.2 Various CCD images obtained during the reduction of optical spectroscopy ............................................................................................................. 50
    • 4.3 An example exposure of an argon calibration lamp used to calibrate the wavelength scale of the science i m a g e s .............................................. 52
    • 4.4 The residual wavelengths from measurements of five prominent sky emission lines and the reduced dispersion of the distribution following co rre c tio n s.......................................................................................................... 53
    • 4.5 Normalised sensitivity functions across the detector, with a magnified view of the 3300-4300 A wavelength r a n g e .............................................. 56
    • 4.6 Residual sensitivity functions from standard star observations from each observing n i g h t ...................................................................................... 57
    • 4.7 The optical spectrum of NGC 4561 before and after the flux calibration 58
    • 5.1 The ultraviolet-infrared colour-mass diagrams for galaxies comprising the total sample, the Virgo cluster and the field environment. AGNhosts and gas deficient galaxies are h ig h lig h ted ........................................
    • 5.2 SDSS images arranged from the bluest to the reddest s p ir a l................
    • 5.3 The relationship between Hi content and ultraviolet-infrared colour .
    • 5.4 The ultraviolet-infrared colour-mass diagram showing the defined boundaries of the transition r e g i o n ..........................................................................
    • 5.5 The morphological type distribution of H R S+ galaxies divided according to their location on the colour-mass d ia g r a m .....................................
    • 5.6 The F U V - H , N U V - B , B - H and F U V - N U V colour-mass diagrams, highlighting the locations of transition region galaxies . . .
    • 5.7 Stellar mass distribution of the transition region galaxies, divided by morphological type and by Hi c o n te n t.........................................................
    • 5.8 The cluster-centric projected-distance and line-of-sight velocity distribution of galaxies in the Virgo cluster r e g io n ...........................................
    • 5.9 The ultraviolet-infrared colour-mass diagram highlighting galaxies for which a stripping timescale estim ate is a v a ila b le .....................................
    • 5.10 SDSS and GALEX images of Hi-normal transition g a la x ie s ................
    • 5.11 SDSS and GALEX images of Hi-normal red-sequence galaxies . . . .
    • 5.12 The M asters et al. (2010) g - r colour-m agnitude diagram compared with a N U V -r diagram for the same sample of g a la x ie s....................
    • 5.13 The distribution of the concentration index in H-band for Virgo cluster g a l a x i e s ...............................................................................................................
    • 5.14 The distribution of the H-band concentration index for Virgo Hi-deficient and Hi-normal transition g a la x ie s ................................................................
    • 8 . 1 Prominent emission line features in the optical spectrum of NGC 4747, including the Hi recombination lines and forbidden lines arising from O, N and S ...................................................................................................... 137
    • 8 . 2 The observed and theoretical relationships between the R23 ratio and the N II/O II and N II/H a r a t i o s .................................................................. 140
    • 8.3 The large discrepancies in the overall shape of M-Z relations derived from different metallicity c a lib ra tio n s ........................................................ 143
    • 8.4 The relationships between the metallicities obtained from the six calibration m e th o d s................................................................................................ 147
    • 8.5 Z-Z relationships with M91 as the base m etallicity .................................. 152
    • 8 . 6 Z-Z relationships with Z94 as the base m e ta llic ity .................................. 153
    • 8.7 Z-Z relationships with D02 as the base m e ta llic ity .................................. 154
    • 8 . 8 Z-Z relationships with PP04 03N2 as the base m etallicity ..................... 155
    • 8.9 Z-Z relationships with PP04 N2 as the base m e ta llic ity ...................... 156
    • 8.10 The distribution of the errors in the final metallicity values, presented for both the D02 and the PP04 base calib ratio n s.................................... 158
    • using D02 and PP04 base calib ratio n s........................................................ 162
    • estim ates derived from single measurements ........................................... 164
    • Oxygen abundance versus the NII/Ho; ratio and the D02 metallicity
    • c a lib ra tio n .......................................................................................................... 165
    • this w o rk ............................................................................................................. 166
    • Abazajian K. N., Adelm an-M cCarthy J. K., Agiieros M. A., Allam S. S., Allende Prieto C., An D., Anderson K. S. J., Anderson S. F., et al. 2009, ApJS, 182, 543
    • Alloin D., Collin-Souffrin S., Joly M., Vigroux L., 1979, A&A, 78, 200
    • Anderson S. F., Voges W., Margon B., Triim per J., Agiieros M. A.,Boiler T., Collinge M. J., Homer L., et al. 2003, AJ, 126, 2209
    • Arnouts S., Walcher C. J., Le Fevre O., Zamorani G., Ilbert O., Le Brun V.,Pozzetti L., Bardelli S., et al. 2007, A&A, 476, 137
    • Athanassoula E., Bosma A., Creze M., Schwarz M. P., 1982, A&A, 107, 101
    • Baes M., Buyle P., Hau G. K. T., Dejonghe H., 2003, MNRAS, 341, L44
    • Baldry I. K., Glazebrook K., Brinkm ann J., Ivezic Z., Lupton R. H., Nichol R. C., Szalay A. S., 2004, ApJ, 600, 681
    • Baldwin J. A., Phillips M. M., Terlevich R., 1981, PASP,93, 5
    • Barth A. J., Ho L. C., Rutledge R. E., Sargent W. L. W., 2004, ApJ, 607, 90
    • Baugh C. M., 2006, Reports on Progress in Physics, 69, 3101
    • Frenk C. S., 1996, MNRAS, 283, 1361
    • Frenk C. S., Lacey C. G., 1998, ApJ, 498,504
    • Bekki K., Couch W. J., 2003, A pJL, 596, L13
    • Bekki K., Couch W. J., Shioya Y., 2002, ApJ, 577, 651
    • Bell E. F., de Jong R. S., 2001, A pJ, 550, 212
    • Bell E. F., McIntosh D. H., K atz N., Weinberg M. D.,2003, ApJS, 149, 289
    • Bell E. F., Zheng X. Z., Papovich C., Borch A., Wolf C., Meisenheimer K., 2007, A pJ, 663, 834
    • B ertola F., Buson L. M., Zeilinger W. W., 1988, Nature, 335, 705
    • B ertola F., Capaccioli M., Oke J. B., 1982, ApJ, 254, 494
    • B ertola F., Corsini E. M., Vega Beltran J. C., Pizzella A., Sarzi M.,Cappellari M., Funes J. G., 1999, A pJL, 519, L127
    • B ettoni D., G alletta G., Sage L. J., 1993, A&A, 280, 121
    • Binggeli B., Cam eron L. M., 1991, A&A, 252, 27
    • Binggeli B., Sandage A., Tam m ann G. A., 1985, AJ, 90, 1681
    • Birnboim Y., Dekel A., Neistein E., 2007, MNRAS, 380, 339
    • B lum enthal G. R., Faber S. M., Primack J. R., Rees M. J., 1984, Nature, 311, 517
    • Bohringer H., Briel U. G., Schwarz R. A., Voges W., H artner G., Triim per J., 1994, N ature, 368, 828
    • Booth C. M., Schaye J., 2010, MNRAS, 405, LI
    • Boselli A., Boissier S., Cortese L., B uat V., Hughes T. M., Gavazzi G., 2009, ApJ, 706, 1527
    • Boselli A., Boissier S., Cortese L., Gavazzi G., 2008, ApJ, 674, 742
    • Boselli A., Boissier S., Cortese L., Gil de Paz A., Buat V., Iglesias-Paramo J.,Madore B. F., Barlow T., et al. 2005, A pJL, 623, L13
    • Boselli A., Boissier S., Cortese L., Gil de Paz A., Seibert M., Madore B. F., Buat V., M artin D. C., 2006, A pJ, 651, 811
    • Boselli A., Cortese L., Deharveng J. M., Gavazzi G., Yi K. S., Gil de Paz A., Seibert M., Boissier S., Donas J., Lee Y., M adore B. F., M artin D. C., Rich R. M., Sohn Y., 2005, ApJL, 629, L29
    • Boselli A., Eales S., Cortese L., Bendo G., Chanial P., B uat V., Davies J., Auld R., et al. 2010, PASP, 122, 261
    • Boselli A., Gavazzi G., 2006, PASP, 118, 517
    • Boselli A., Gavazzi G., Donas J., Scodeggio M., 2001, AJ, 121, 753
    • Boselli A., Gavazzi G., Franzetti P., Pierini D., Scodeggio M., 2000, A&AS, 142, 73
    • Boselli A., Lequeux J., Gavazzi G., 2002, A&A, 384, 33
    • Boselli A., Sauvage M., Lequeux J., Donati A., Gavazzi G., 2003, A&A, 406, 867
    • Boselli A., Tuffs R. J., Gavazzi G., Hippelein H., Pierini D., 1997, A&AS, 121, 507
    • Bower R. G., Benson A. J., M albon R., Helly J. C., Frenk C. S., Baugh C. M., Cole S., Lacey C. G., 2006, MNRAS, 370, 645
    • Bravo-Alfaro H., Cayatte V., van Gorkom J. H., Balkowski C., 2000, AJ, 119, 580
    • Bresolin F., 2006, ArXiv astro-ph/0608410
    • Bridle A. H., Hough D. H., Lonsdale C. J., Burns J. O., Laing R. A., 1994, AJ, 108, 766
    • Brown W. R., Geller M. J., Kenyon S. J., K urtz M. J., 2006, ApJ, 647, 303
    • Bruzual G., Chariot S., 2003, MNRAS, 344, 1000
    • Cayatte V., Kotanyi C., Balkowski C., van Gorkom J. H., 1994, AJ, 107, 1003
    • Cayatte V., van Gorkom J. H., Balkowski C., Kotanyi C., 1990, AJ, 100, 604
    • Code A. D., 1969, PASP, 81, 475
    • Cole S., Lacey C., 1996, MNRAS, 281, 716
    • Cole S., Norberg P., Baugh C. M., Frenk C. S., Bland-Hawthorn J., Bridges T., Cannon R., Colless M., et al. 2001, MNRAS, 326, 255
    • Colless M., Dalton G., M addox S., Sutherland W., Norberg P., Cole S., BlandHawthorn J., Bridges T., et al. 2001, MNRAS, 328, 1039
    • Cortese L., Boselli A., B uat V., Gavazzi G., Boissier S., Gil de Paz A., Seibert M., Madore B. F., M artin D. C., 2006, A pJ, 637, 242
    • Cortese L., Boselli A., Franzetti P., Decarli R., Gavazzi G., Boissier S., B uat V., 2008, MNRAS, 386, 1157
    • Cortese L., Boselli A., Gavazzi G., Iglesias-Param o J., Madore B. F., Barlow T., Bianchi L., Byun Y., et al. 2005, A pJL, 623, L17
    • Cortese L., Davies J. I., Pohlen M., et al. 2010, A&A, 518, L49+
    • Cortese L., Gavazzi G., Boselli A., F ranzetti P., K ennicutt R. C., O 'Neil K., Sakai S., 2006, A&A, 453, 847
    • Cortese L., Hughes T. M., 2009, MNRAS, 400, 1225
    • Cowie L. L., Songaila A., 1977, N ature, 266, 501
    • Croton D. J., Springel V., W hite S. D. M., De Lucia G., Frenk C. S., Gao L., Jenkins A., Kauffmann G., Navarro J. F., Yoshida N., 2006, MNRAS, 365, 11
    • Crowl H. H., Kenney J. D. P., 2008, A J, 136, 1623
    • Cutri R. M., Nelson B. O., Francis P. J., Sm ith P. S., 2002, in R. F. Green, E. Y. Khachikian, & D. B. Sanders ed., IAU Colloq. 184: AGN Surveys Vol. 284 of Astronomical Society of the Pacific Conference Series, The 2MASS Red AGN Survey, pp 127-I-
    • Dalla Vecchia C., Bower R. G., Theuns T., Balogh M. L., M azzotta P., Frenk C. S., 2004, MNRAS, 355, 995
    • Dave R., Oppenheimer B. D., 2007, MNRAS, 374, 427
    • Davis M., Efstathiou G., Frenk C. S., W hite S. D. M., 1985,ApJ, 292, 371
    • de Blok W. J. G , McGaugh S. S., 1998, A pJ, 508, 132
    • De Lucia G., Kauffmann G., W hite S. D. M., 2004, MNRAS, 349, 1101
    • de Rossi M. E., Tissera P. B., Scannapieco C., 2007, MNRAS, 374, 323
    • Decarli R., Gavazzi G., Arosio I., Cortese L., Boselli A., Bonfanti C., Colpi M., 2007, MNRAS, 381, 136
    • Denicolo G., Terlevich R., Terlevich E., 2002, MNRAS, 330, 69
    • Desai V., Dalcanton J. J., Aragon-Salamanca A., Jablonka P., Poggianti B., Gogarten S. M., Simard L., Milvang-Jensen B., Rudnick G., Zaritsky D., Clowe D., Halliday C., Pello R., Saglia R., W hite S., 2007, A pJ, 660, 1151
    • Diaz A. I., Perez-Montero E., 2000, MNRAS, 312, 130
    • Dopita M. A., Evans I. N., 1986, A pJ, 307, 431
    • Dors Jr. O. L., Copetti M. V. F., 2006, A&A, 452, 473
    • Draine B. T., Dale D. A., Bendo G., Gordon K. D., Smith J. D. T., Armus L., Engelbracht C. W., Helou G., et al. 2007, A pJ, 663, 866
    • Dressier A., Oemler Jr. A., Couch W. J., Smail I., Ellis R. S., Barger A., Butcher H., Poggianti B. M., Sharpies R. M., 1997, A pJ, 490, 577
    • Edm unds M. G., Pagel B. E. J., 1984, MNRAS, 211, 507
    • Ellison S. L., Sim ard L., Cowan N. B., Baldry I. K., P atton D. R., McConnachie A. W., 2009, MNRAS, 396, 1257
    • Elmegreen B. G., B ournaud F., Elmegreen D. M., 2008, ApJ, 688, 67
    • Erb D. K., Shapley A. E., P ettini M., Steidel C. C.,Reddy N. A.,Adelberger K. L., 2006, A pJ, 644, 813
    • Faber S. M., W illmer C. N. A., Wolf C., Koo D. C., Weiner B. J., Newman J. A., Im M., Coil A. L., Conroy C., 2007, ApJ, 665, 265
    • Ferland G. J., K orista K. T., Verner D.A., Ferguson J. W.,Kingdon J. B.,Verner E. M., 1998, PASP, 110, 761
    • Ferrarese L., Ford H., 2005, Space Sci. Rev., 116, 523
    • Ferrarese L., M erritt D., 2000, A pJL, 539, L9
    • Fine S., Croom S. M., Miller L., Babic A., Moore D., Brewer B., Sharp R. G., Boyle B. J., Shanks T., Sm ith R. J., O utram P. J., Loaring N. S., 2006, MNRAS, 373, 613
    • Fioc M., Rocca-Volmerange B., 1997, A&A, 326, 950
    • Forman W., Jones C., Churazov E., M arkevitch M., Nulsen P., Vikhlinin A., Begelm an M., Bohringer H., Eilek J., Heinz S., K raft R., Owen F., Pahre M., 2007, ApJ, 665, 1057
    • Frayer D. T., Brown R. L., 1997, A pJS, 113, 221
    • G arnett D. R., Shields G. A., Skillman E. D., Sagan S. P., Dufour R. J., 1997, ApJ, 489, 63
    • Gavazzi G., 1989, ApJ, 346, 59
    • Gavazzi G., Bonfanti C., Sanvito G., Boselli A., Scodeggio M., 2002, ApJ, 576, 135
    • Gavazzi G., Boselli A., Donati A., Franzetti P., Scodeggio M ., 2003a, A&A, 400, 451
    • Gavazzi G., Boselli A., Donati A., Franzetti P., Scodeggio M ., 2003b, A&A, 400, 451
    • Gavazzi G., Boselli A., Scodeggio M., Pierini D., Belsole E ., 1999, MNRAS, 304, 595
    • Gavazzi G., Franzetti P., Scodeggio M., Boselli A., P ierini D ., Baffa C., Lisi F., Hunt L. K., 2000, A&AS, 142, 65
    • Gavazzi G., Zaccardo A., Sanvito G., Boselli A., B onfanti C., 2004, A&A, 417, 499
    • Geller M. J., Huchra J. P., 1989, Science, 246, 897
    • Georgakakis A., Nandra K., Yan R., Willner S. P., Lotz J. M ., Pierce C. M., Cooper M. C., Laird E. S., Koo D. C., Barmby P., Newman J. A., Primack J. R., Coil A. L., 2008, MNRAS, 385, 2049
    • Ghigna S., Moore B., Governato F., Lake G., Q uinn T ., S tad el J., 1998, MNRAS, 300, 146
    • Gil de Paz A., Boissier S., Madore B. F., Seibert M., Jo e Y. H., Boselli A., W yder T. K., et al. 2007, ApJS, 173, 185
    • Girardi M., Giuricin G., M ardirossian F., M ezzetti M., B oschin W., 1998, ApJ, 505, 74
    • Glazebrook K., Blake C., Couch W ., Forbes D., D rinkw ater M ., Jurek R., Pimbblet K., Madore B., M artin C., Small T., Forster K., Colless M ., Sharp R., Croom S., Woods D., Pracy M., Gilbank D., Yee H., Gladders M ., 2007, in N. Metcalfe & T. Shanks ed., Cosmic Frontiers Vol. 379 of A stronom ical Society of the Pacific Conference Series, The WiggleZ Project: AAOmega a n d D a rk Energy, pp 72-|-
    • Gordon K. D., Clayton G. C., W itt A. N., Misselt K. A., 2000, A pJ, 533, 236
    • Griffin M. J., Abergel A., Abreu A., Ade P. A. R., A ndre P., Augueres J., Babbedge T., Bae Y., et al. 2010, A&A, 518, L3+
    • Gunn J. E., G ott J. R. I., 1972, A pJ, 176, 1
    • Haines C. P., G argiulo A., Merluzzi P., 2008, MNRAS, 385, 1201
    • Hau G. K. T., Bower R. G., Kilborn V., Forbes D. A., Balogh M. L., Oosterloo T., 2008, MNRAS, 385, 1965
    • Haynes M. P., Giovanelli R., 1984, AJ, 89, 758
    • Haynes M. P., Jore K. P., B arrett E. A., Broeils A. H., M urray B. M., 2000, AJ, 120, 703
    • Heckman T. M., Kauffm ann G., Brinchmann J., Chariot S., Tremonti C., W hite S. D. M., 2004, A pJ, 613, 109
    • Henry R. B. C., Pagel B. E. J., Chincarini G. L., 1994, MNRAS, 266, 421
    • Henry R. B. C., Pagel B. E. J., Lasseter D. F., Chincarini G. L., 1992, MNRAS, 258, 321
    • Hernan-Caballero A., Perez-Fournon I., Hatziminaoglou E., Afonso-Luis A., RowanRobinson M., Rigopoulou D., Farrah D., Lonsdale C. J., et al. 2009, MNRAS, 395, 1695
    • Hummel E., van der Hulst J. M., K ennicutt R. C., Keel W. C., 1990, A&A, 236, 333
    • Hunt L. K., Thuan T. X., Izotov Y. I., Sauvage M., 2010, ApJ, 712, 164
    • Hunter S. D., Bertsch D. L., Catelli J. R., Dame T. M., Digel S. W., Dingus B. L., Esposito J. A., Fichtel C. E., et al. 1997, ApJ, 481, 205
    • Iglesias-Paramo J., Buat V., Takeuchi T. T., Xu K., Boissier S., Boselli A., Burgarella D., Madore B. F., et al. 2006, ApJS, 164, 38
    • K ennicutt Jr. R. C., 1983, A J, 88, 483
    • K ennicutt Jr. R. C., 1992, A pJ, 388, 310
    • K ennicutt Jr. R. C., 1998, ARA&A, 36, 189
    • K ennicutt Jr. R. C., Armus L., Bendo G., Calzetti D., Dale D. A., Draine B. T., Engelbracht C. W ., Gordon K. D., et al. 2003, PASP, 115, 928
    • K ennicutt Jr. R. C., R oettiger K. A., Keel W. C., van der Hulst J. M., Hummel E., 1987, AJ, 93, 1011
    • K ennicutt Jr. R. C., Tam blyn P., Congdon C. E., 1994, A pJ, 435, 22
    • Kewley L. J., D opita M. A., 2002, ApJS, 142, 35
    • Kewley L. J., D opita M. A., Sutherland R. S., Heisler C. A., Trevena J., 2001, ApJ, 556, 121
    • Kewley L. J., Ellison S. L., 2008, A pJ, 681, 1183
    • Kobulnicky H. A., K ennicutt Jr. R. C., Pizagno J. L., 1999, A pJ, 514, 544
    • Kobulnicky H. A., Kewley L. J., 2004, A pJ, 617, 240
    • Kobulnicky H. A., Zaritsky D., 1999, A pJ, 511, 118
    • K odam a T., Yam ada T., Akiyam a M., Aoki K., Doi M., Furusawa H., Fuse T., Imanishi M., et al. 2004, MNRAS, 350, 1005
    • Kronberger T., Kapferer W., Ferrari C., Unterguggenberger S., Schindler S., 2008, A&A, 481, 337
    • Kroupa P., Tout C. A., Gilmore G., 1993, MNRAS, 262, 545
    • Krumholz M. R., McKee C. F., Tumlinson J., 2009, A pJ, 693, 216
    • Krumm N., van Driel W., van Woerden H., 1985, A&A, 144, 202
    • Lamareille F., Mouhcine M., Contini T., Lewis I., Maddox S., 2004, MNRAS, 350, 396
    • Lamastra A., Bianchi S., M att G., Perola G. C., Barcons X., Carrera F. J., 2009, A&A, 504, 73
    • Larson R. B., Tinsley B. M., Caldwell C. N., 1980, A pJ, 237, 692
    • Laurent O., Mirabel I. F., Charm andaris V., Gallais P., M adden S. C., Sauvage M., Vigroux L., Cesarsky C., 2000, A&A, 359, 887
    • Lee S., Irwin J. A., 1997, ApJ, 490, 247
    • Leitherer C., Schaerer D., Goldader J. D., Gonzalez Delgado R. M., Robert C., Kune D. F., de Mello D. F., Devost D., Heckman T. M., 1999, ApJS, 123, 3
    • Lemaitre G., Kohler D., Lacroix D., Meunier J. P., Vin A., 1990, A&A, 228, 546
    • Lequeux J., Peimbert M., Rayo J. F., Serrano A., Torres-Peimbert S., 1979, A&A, 80, 155
    • Liang Y. C., Yin S. Y., Hammer F., Deng L. C., Flores H., Zhang B., 2006, ApJ, 652, 257
    • Lilly S. J., Le Fevre O., Hammer F., C ram pton D., 1996, ApJL, 460, L1+
    • Lintott C. J., Schawinski K., Slosar A., Land K., Bamford S., Thomas D., Raddick M. J., Nichol R. C., Szalay A., Andreescu D., M urray P., Vandenberg J., 2008, MNRAS, 389, 1179
    • Liu X., 2002, in W. J. Henney, J. Franco, & M. M artos ed., Revista Mexicana de Astronomia y Astrofisica Conference Series Vol. 12 of Revista Mexicana de Astronomia y Astrofisica Conference Series, Optical Recombination Lines and Temperature Fluctuations, pp 70-76
    • Maccio A. V., Moore B., Stadel J., 2006, A pJL, 636, L25
    • M adau P., Ferguson H. C., Dickinson M. E., Giavalisco M., Steidel C. C., Fruchter A., 1996, MNRAS, 283, 1388
    • M agorrian J., Trem aine S., Richstone D., Bender R., Bower G., Dressier A., Faber S. M., G ebhardt K., Green R., G rillm air C., Kormendy J., Lauer T., 1998, AJ, 115, 2285
    • Mannucci F., Cresci G., Maiolino R., Marconi A., Gnerucci A., 2010, ArXiv astrop h / 10050006
    • McNamara B. R., Nulsen P. E. J., 2007, ARA&A, 45, 117
    • Mehlert D., Noll S., Appenzeller I., Saglia R. P., Bender R., Bohm A., Drory N., Pricke K., Gabasch A., Heidt J., Hopp U., Jager K., Mollenhoff C., Seitz S., Stahl O., Ziegler B., 2002, A&A, 393, 809
    • Melendez M., Kraemer S. B., A rm entrout B. K., Deo R. P., Crenshaw D. M., Schmitt H. R., Mushotzky R. F., Tueller J., M arkwardt C. B., W inter L., 2008, ApJ, 682, 94
    • Mouhcine M., Bamford S. P., Aragon-Salam anca A., Nakam ura O., Milvang-Jensen B., 2006, MNRAS, 369, 891
    • Mouhcine M., Gibson B. K., R enda A., K aw ata D., 2008, A&A, 486, 711
    • Moustakas J., K ennicutt Jr. R. C., 2006, A pJS, 164, 81
    • Moustakas J., K ennicutt Jr. R. C., Trem onti C. A., Dale D. A., Sm ith J., Calzetti D., 2010, A pJS, 190, 233
    • Pagel B. E. J., Edmunds M. G., Smith G., 1980, MNRAS, 193, 219
    • Pagel B. E. J., Patchett B. E., 1975, MNRAS, 172, 13
    • Panuzzo P., Bressan A., G ranato G. L., Silva L., Danese L., 2003, A&A, 409, 99
    • Patil M. K., Pandey S. K., Kembhavi A., Sahu D. K., 2009, ArXiv astro-ph/09011747
    • Peebles P. J. E., 1969, ApJ, 155, 393
    • Quilis V., Moore B., Bower R., 2000, Science, 288, 1617
    • Schodel R., O tt T., Genzel R., Eckart A., M ouawad N., Alexander T., 2003, ApJ, 596, 1015
    • Searle L., Sargent W. L. W., 1972, A pJ, 173, 25
    • Stasinska G., Asari N. V., Fernandes R. C., Gomes J. M., Schlickmann M., Mateus A., Schoenell W., Sodre Jr. L., 2008, MNRAS, 391, L29
    • Storchi-Bergmann T., C alzetti D., Kinney A. L., 1994, ApJ, 429, 572
    • Sutherland R. S., D opita M. A., 1993, ApJS, 88, 253
    • Tecce T. E., Cora S. A., Tissera P. B., Abadi M. G., Lagos C. d. P., 2010, ArXiv ast ro-ph /10065446
    • Tonnesen S., Bryan G. L., 2009, ApJ, 694, 789
    • Tremonti C. A., Heckman T. M., Kauffmann G., Brinchmann J., Chariot S., W hite S. D. M., Seibert M., Peng E. W., Schlegel D. J., Uomoto A., Fukugita M., B rinkm ann J., 2004, A pJ, 613, 898
    • Wang J., Fabbiano G., R isaliti G., Elvis M., Mundell C.G., Dum as G., Schinnerer E., Zezas A., 2010, ApJL, 719, L208
  • No related research data.
  • No similar publications.

Share - Bookmark

Cite this article